Hostname: page-component-cd9895bd7-jkksz Total loading time: 0 Render date: 2024-12-23T06:27:45.878Z Has data issue: false hasContentIssue false
  • English
  • Français

Jet-linked X-ray emission in radio-loud broad absorption line (BAL) quasars

Published online by Cambridge University Press:  21 February 2013

M. Kunert-Bajraszewska ,
K. Katarzyński ,
A. Janiuk  and
M. Cegłowski
M. Kunert-Bajraszewska
Affiliation:
Toruń Centre for Astronomy, N. Copernicus University, Gagarina 11, 87-100 Toruń, Poland email: [email protected]
K. Katarzyński
Affiliation:
Toruń Centre for Astronomy, N. Copernicus University, Gagarina 11, 87-100 Toruń, Poland email: [email protected]
A. Janiuk
Affiliation:
Center for Theoretical Physics, PAS, Al.Lotnikow 32/46, 02-668 Warsaw, Poland
M. Cegłowski
Affiliation:
Toruń Centre for Astronomy, N. Copernicus University, Gagarina 11, 87-100 Toruń, Poland email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We have applied theoretical models to explain spectral energy distribution (SED) of three radio-loud broad absorption line (BAL) quasars: an extended hybrid object PG 1004+130 and two compact sources 1045+352 and 3C270.1. We calculate the emission from the very inner part of the sources which accounts for more than 90% of the observed X-ray radiation. In our analysis we consider a scenario in which the observed X-ray emission comes from the inverse-Compton (IC) scattering inside a jet and from the accretion disk corona. The compact objects 1045+352 and 3C270.1 are high-redshift quasars (z = 1.604 and 1.532 respectively), with strong radio cores. We argue that in the case of these two sources a non-thermal, inverse-Compton emission from the innermost parts of the jet can explain a large fraction of the observed X-ray emission. The large scale object PG 1004+130 with a peculiar radio morphology is a low-redshift (z = 0.24), lobe-dominated BAL quasar with a weak radio core. In this case simulated inverse-Compton X-ray emission of the jet is relatively low. However, the corona emission appears strong enough to explain the observed X-ray spectrum of this object.

Keywords

Physical data and processes: accretionquasars: individual (1045+352, 3C270.1, PG 1004+130)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S290: Feeding Compact Objects: Accretion on All Scales , August 2012 , pp. 243 - 244
Copyright
Copyright © International Astronomical Union 2013

References

Kunert-Bajraszewska, M., Siemiginowska, A., Katarzyski, K., & Janiuk, A., 2009, ApJ, 705, 1356CrossRefGoogle Scholar
Miller, B. P.et al., 2009, ApJ, 702, 911CrossRefGoogle Scholar
Stocke, J. T., Morris, S. L., Weymann, J. T., & Foltz, C. B., 1992, ApJ, 396, 487CrossRefGoogle Scholar
Worrall, D. M., Tananbaum, H., Giommi, P., & Zamorani, G., 1987, ApJ, 313, 596Google Scholar
Zamorani, G.et al., 1981, ApJ, 245, 357CrossRefGoogle Scholar